0Assigned ID: 2377
----- Attempting Submission 1 (Fri Apr 09 22:45:18 GMT 2021) -----
HST Phase I Proposal 2377 successfully submitted.
Receipt: # 2377-1
----- Attempting Submission 2 (Fri Apr 09 23:16:30 GMT 2021) -----
HST Phase I Proposal 2377 successfully submitted.
Receipt: # 2377-2
----- Attempting Submission 3 (Fri Apr 09 23:51:08 GMT 2021) -----FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.New update (08/03/23): I added visit 15 and 16, that are the repetitions of the second and third orbit of Visit 09 and of the first orbit of Visit10, respectively. These observations are needed to complete the box dithering pattern of the STIS/NUV-MAMA F25CIII observations for the target J104457, thus I specified for each exposure the X and Y POS TARG. We require that the repeat observations are performed with the same orient of the observations of Visit 09 and Visit 10.
New update (04/09/23): I added visit 14, that is the repetition of the first orbit of Visit 06 using the filter STIS/NUV-MAMA F25CIII for the target SBS-0335-052. We require that the repeat observations are performed with the same orient of the observations of Visit 06, taken on 03/18/23.
New update (11/22/22): I added visit 13, that is the repetition of the failed first orbit of Visit 02, using the filters F150LP and F165LP for the target J141851. We require that the repeat observations are performed with the same orient of the observations of Visit 02 taken on 08/24/22.
New update (04/07/22): I added visit 12, that is the repetition of the failed second orbit of Visit 08, using the filters F125LP and F140LP for the target J04457. We packed the two orbits of visit 08 using our own sub-pixel dithering pattern using POS-TARGs and asking the special constraint SHADOW. We divided the exposure time of each filter in 4 exposures in a way that the SHADOW part of the orbit is covered by the F125LP filter, while the remaining parts are used for the observations with the F140LP filter. We require that the repeat observations of the second orbit are performed with the same orient and special constraints of the observations of the first orbit of Visit 08 taken on 02/19/22.
New update (12/22): I am resubmitting to correct the target of Visit 8, that is J104457 instead of J141852.
New update (09/08): I am resubmitting, after setting a post-flash of 20 to avoid too low background for the WFC3 UVIS filters that needed that, as suggested by Mireia Montes. Let me know if there are further things to fix. Thank you!
Update: I am resubmitting because closing and opening again the APT, cancelling the cache of the visit planner, and running again all the tools, I could solve the problem of the visit planner for the WFC3 observations of the source SBS-0335-052, that now is schedulable. The issue with the
BOT and the warnings for the WFC3/UVIS filters instead are still there.
Dear Christian and Svea,
I would really appreciate if you could check the dithering pattern that I manually created for the ACS/SBC observations for J1044 and J1418. Indeed, we required the special requirement SHADOW for the F125LP filter, and so to avoid to loose exposure time because of the reduced orbits,
we packed the visits using our own sub-pixel dithering pattern using POS-TARGs, in a way that the SHADOW part of the orbit is covered by the F125LP filter, while the remaining part is used for the observations with the other ACS/SBC filters. Specifically, we divided the exposure time of
each filter in 4 exposures, shifting each exposure in diagonal of 7.5 pixels (that correspond to XPOS = 2.252” and YPOS=0.2505”) creating a box around the central coordinates of the targets. Our aim is to avoid problems due to the dead column of SBC (~5 pixels wide), but also to try to
improve the spatial sampling of the final maps.
Finally, I run the BOT and I noticed problems in 5 visits (in visit 06 and 10 with STIS, and in visit 05 with WFC3), while for visit 07 and 11 with the filter FQ492 of WFC3 there is the message that the observation is not supported, but without explaining why. Let me know how I can solve these
problems.
Thank you very much in advance.
Best,
Matilde524689816----- Attempting Submission 1 (Fri Jul 30 01:46:47 GMT 2021) -----
HST Phase II Proposal 16763 successfully submitted.
Receipt: # 16763-1
----- Attempting Submission 2 (Fri Jul 30 04:38:25 GMT 2021) -----
----- Attempting Submission 3 (Wed Sep 08 17:33:23 GMT 2021) -----
----- Attempting Submission 4 (Wed Dec 22 05:53:53 GMT 2021) -----
----- Attempting Submission 5 (Fri Apr 08 03:04:47 GMT 2022) -----
----- Attempting Submission 6 (Tue Nov 22 15:06:18 GMT 2022) -----
----- Attempting Submission 7 (Sun Apr 09 16:36:38 GMT 2023) -----
----- Attempting Submission 8 (Thu Aug 03 19:05:30 GMT 2023) -----For this resubmission I have just added visit 15 and 16 to repeat failed observations with STIS/NUV-MAMA F25CIII. The errors reported here are not related to this last modification.
Let me know if something is not correct.
Thank you very much!
MatildeTracking down the origin of UV photons in local high-z analogues with FUV emission line imagingFar ultraviolet emission lines are fundamental to interpret the ionized interstellar medium (ISM) properties of the first generation of galaxies that will be observed with the James Webb Space Telescope (JWST). The COS Legacy Archive Spectroscopic SurveY (CLASSY) HST/COS treasury program provided the first high-resolution spectral catalog of local high-z analogues to investigate their stellar and gas properties to improve the diagnostic power of UV lines. However, in order to fully understand the physical conditions that give rise to their excitation, we need to spatially tackle these diagnostics. This will allow us to trace their spatial distribution and to isolate the origin of the UV photons within these systems. Here we propose to obtain emission line images down to ~10 pc resolution, using the high resolution imaging from ACS and STIS, of three nearby well-known low-metallicity starbursts selected from CLASSY. These sources are remarkably characterized by strong CIV1548,1551, HeII1640, [OIII]1661,6 and [CIII]1907,CIII]1909, and by different Ly-alpha profiles. The powerful combination of available optical integral field spectroscopy data, archival and new HST observations in concert with state-of-the-art models will allow us to investigate and interpret the morphology of the emission line diagnostics. Hence, not only we will be able to track the ionization source(s) of the gas and the ionization structure in our targets, but also test indirect tracers of leaking ionizing radiation (i.e., Lyman continuum escape). This study will provide us with an extremely powerful toolkit, pivotal for understanding the ISM conditions of the earliest galaxies.The goal of this proposal is to map with ACS/SBC and STIS/NUV the extended Ly alpha, CIV, HeII1640+[OIII]1661,6 and CIII]1907,09 to compare their morphologies and study their line ratios with spatial resolution down to ~10 pc in three local extreme galaxies:
1) J1418+2102
2) J1044+0353
3) SBS 0335-052.
Target 1: we request ACS/SBC F125LP, F140LP, F150LP and F165LP to cover Ly alpha, FUV continuum, CIV1548,51 and HeII1640+[OIII]1661,6, respectively. We additionally request STIS/NUV F25CIII to isolate CIII]. WFC3/UVIS F336W, F438W, F606W and F814W filters, combined with with STIS/NUV F25QTZ and ACS/SBC F140LP filters, will be used to model the stellar spectral energy distribution (SED). Finally, we will exploit archival data for Halpha and Hbeta imaging.
Target 2 and 3: both have ongoing observations to perform CIV1548,51, HeII1640 and [OIII]1661,6 imaging (PID: 16209). For SBS0335-052, Lyalpha imaging has been already performed by Ostlin+2009. Moreover, these two sources have already all the necessary broad-band optical imaging, including Halpha. As such, here we request only WFC3/UVIS FQ492N to cover Hbeta, STIS/NUV F25CIII and F25QTZ to isolate CIII]1907,09 for both targets. For target 2, we request also ACS/SBC F125LP and F140LP to isolate Ly alpha.
We expect that the targeted emission will be well captured in one pointing of the ACS/SBC (34.6"x30") and STIS/NUV (25"x25"), with sufficient space for background subtraction.
ETCs: In order to estimate exposure times, we took advantage of each target's archival COS spectrum, from which we measured the stellar continuum and emission line surface brightnesses in the COS aperture (2.5"x2.5"). We used these values as input for the ACS and STIS Exposure Time Calculators (ETC). For the WFC3 optical filters, we estimated the continuum and Hbeta surface brightness from the MUSE data, extracting a spectrum from a region comparable to the COS aperture. Moreover, we assumed that the targeted line emission is coming from an extended region with an aperture of 2.5".
ACS/SBC observations:
The F125LP filter omits the bright geocoronal Ly-alpha background, but unfortunately includes the geocoronal line OI1302. Therefore, we require the special requirement SHADOW just for the F125LP filter. We packed the visits using our own sub-pixel dithering pattern using POS-TARGs, dividing the exposure time of each filter in 4 exposures in a way that the SHADOW part of the orbit is covered by the F125LP filter, while the remaining parts are used for the observations with the other ACS/SBC filters.
STIS/NUV observations:
For the STIS dithering strategy we selected the box pattern, dividing each exposure in 4 sub-exposures. For target 1 and target 2, we divided the observations in two visits to avoid visits longer than 5 orbits.
WFC3/UVIS:
For the WFC3 dithering strategy we selected the 3-point pattern, dividing each filter exposure into 3 sub-exposures.All the members of the team are experts in observational studies of starburst galaxies, particularly focusing on nebular gas and its diagnostics.
Scientifically, the team is uniquely qualified to pursue the broad range of science topics proposed here.
Our team contain forefront leaders in UV and optical diagnostics (Berg, James, Mingozzi, Aloisi, Arellano-Cordova, Erb, Brinchmann, Nanayakkara, Martin, Maseda, Hayes, Gazagnes, Hirschauer, Nanayakkara, Kumari), and Ly-alpha analysis (Erb, Hayes, Henry, Martin, Gazagnes).
Our Co-Is have extensive expertise in emission line modeling using photoionization codes such as CLOUDY and mappings (Berg, Erb, James, Arellano-Cordova, Nanayakkara, Amorin, Martin, Hernandez)
and in stellar evolution modeling (Brinchmann, Chisholm, Wofford).
We also have significant expertise in imaging with Hubble (Hayes, Aloisi, Wofford). M. Hayes pioneered the use of ACS/SBC to image ultraviolet emission lines at low-redshift, starting with Ly-alpha (Hayes+2005, 2007, 2013, 2014). 15 refereed papers in total have been based on these methods, including a dedicated paper on the methods (Hayes+2009).
Our team is balanced with both pioneers of UV spectroscopy as well as new experts in the field. The team is also anchored at both low-redshift and high-redshift such that we will design the proposed UV emission-line diagnostics with an eye towards what is observable by JWST.Galaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSTARBURSTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ACS/SBCImagingNoNoF125LPACS/SBCImagingNoNoF140LPACS/SBCImagingNoNoF150LPACS/SBCImagingNoNoF165LPSTIS/NUV-MAMAImagingNoNoF25CIIISTIS/NUV-MAMAImagingNoNoF25QTZWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WSTIS/NUV-MAMAImagingNoNoF25CIIISTIS/NUV-MAMAImagingNoNoF25QTZWFC3/UVISImagingNoNoFQ492NACS/SBCImagingNoNoF125LPACS/SBCImagingNoNoF140LPSTIS/NUV-MAMAImagingNoNoF25CIIISTIS/NUV-MAMAImagingNoNoF25QTZWFC3/UVISImagingNoNoFQ492NPOS-TARGDITHER0.275LINE0.275falsefalse143.130102426.6STIS-MAMA-BOX2falsePOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT5falseThe scheduling data was generated by CASM 31.0.CASM was run in Phase II mode./private/var/folders/3m/wvp8cnz55q558ygnl0kddrzh0002nx/T/OPVisit563534447666058143.xml1649582842000232.0(Tic-Visit
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